Talk abstract details

The Be stars HD181231(B5IVe) and HD175869 (B8IIIe) have recently been observed using the CoRoT satellite for $\sim$ 5 months and $\sim$ 27 days respectively. This continuous, space-based observation has allowed the detection of many low amplitude modes in these stars. In the case of HD181231, the combination of the CoRoT data and ground based spectroscopic follow-up data have placed tight constraints on the fundamental and pulsational properties of this star, allowing for detailed seismic modelling.
For HD175869, the variability has been proposed to be the result of inhomogeneities produced by stellar activity, located in or just above the photosphere. However, the CoRoT data does not allow non-radial pulsations to be excluded as the origin of the variability. Seismic modelling of this star will clarify this issue.
We have compared the observed frequencies to those calculated using 2D stellar evolution and a 2D linear adiabatic pulsation code. We will also discuss compare our results to frequencies calculated using a 1D non-adiabatic pulsation code. Using a combination of frequencies, we have been able to constrain the rotation and extra mixing for stars of a known mass and age. Here we extend this method to determine the best fitting mass, age, rotation rate and amount of extra mixing for these Be stars.